Six detached white-dwarf close binaries

Morales-Rueda, L.; Marsh, T. R.; Maxted, P. F. L.; Nelemans, G.; Karl, C.; Napiwotzki, R.; Moran, C.

doi:10.1111/j.1365-2966.2005.08943.x

Cited by 58 publications

(50 citation statements)

References 86 publications

(118 reference statements)

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“…Liebert et al (2005) noted the absence of non-accreting magnetic white dwarfs (MWDs) among the more than 1200 WDMS binaries compiled by Silvestri et al (2007) and various other samples (Marsh 2000;Ritter & Kolb 2003;Schreiber & Gänsicke 2003;Morales-Rueda et al 2005;Shimansky et al 2006). MWDs are clearly underrepresented in current WDMS samples compared to the ∼10% fraction in the field (Liebert et al 2003).…”

Section: Discussionmentioning

confidence: 99%

Post common envelope binaries from the SDSS

Schwope¹,

Gómez‐Morán²,

Schreiber

et al. 2009

A&A

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We report the discovery of the ninth pre-polar consisting of a late-type ZAMS secondary and a magnetic white dwarf. The white dwarf accretes at an extreme low rate,Ṁ ∼ 10 −14 M yr −1 , from the wind of the companion donor star. The source was found in our systematic search for WD/MS binaries within SDSS/SEGUE. Based on seven Sloan spectra we estimate a binary period of ∼200, 230, or 270 min. The UV to IR spectral energy distribution was decomposed into a dM3-dM4 ZAMS secondary and a cool white dwarf, ∼9000 K, which consistently imply a distance between 360 and 420 pc. The optical spectrum displays one pronounced cyclotron hump, likely originating from a low-temperature plasma, ∼1 keV, in a field of 108 MG. We comment on the evolutionary link between polars and pre-polars.

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Section: Discussionmentioning

confidence: 99%

Post common envelope binaries from the SDSS

Schwope¹,

Gómez‐Morán²,

Schreiber

et al. 2009

A&A

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“…Four more double-degenerates are marked in Table 1 as DD, but were found by independently obtained observations: HE 1511-0448 (Nelemans et al 2005), WD 1241-010 (Marsh et al 1995), WD 1022+050 and WD 2032+188 (Morales-Rueda et al 2005).…”

Section: Double-degenerate White Dwarfsmentioning

confidence: 99%

High-resolution UVES/VLT spectra of white dwarfs observed for the ESO SN Ia Progenitor Survey

Koester¹,

Voß

Napiwotzki

et al. 2009

A&A

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Context. The ESO Supernova Ia Progenitor Survey (SPY) took high-resolution spectra of more than 1000 white dwarfs and pre-white dwarfs. About two thirds of the stars observed are hydrogen-dominated DA white dwarfs. Here we present a catalog and detailed spectroscopic analysis of the DA stars in the SPY. Aims. Atmospheric parameters effective temperature and surface gravity are determined for normal DAs. Double-degenerate binaries, DAs with magnetic fields or dM companions, are classified and discussed. Methods. The spectra are compared with theoretical model atmospheres using a χ 2 fitting technique. Results. Our final sample contains 615 DAs, which show only hydrogen features in their spectra, although some are double-degenerate binaries. 187 are new detections or classifications. We also find 10 magnetic DAs (4 new) and 46 DA+dM pairs (10 new).

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“…To explore the parameter space we enlarged the sample by taking the PCEB lists of Morales-Rueda et al (2005) and Shimansky et al (2006), examined the published data on these systems, and included HS 1857+5144 (Aungwerojwit et al 2007). Since our main interest concerns potential precataclysmic variables such as LTT 560, we limited the sample to PCEBs with P orb < 1 d that contain a white dwarf as primary component.…”

Section: Discussionmentioning

confidence: 99%

Multiple emission line components in detached post-common-envelope binaries

Tappert

Gänsicke

Rebassa‐Mansergas

et al. 2011

A&A

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Motivated by the recent discovery of an Hα emission line component originating close to the white dwarf primary in the post-commonenvelope binary (PCEB) LTT 560, we have undertaken a spectroscopic snapshot survey on 11 short-period (P orb < 6 h) PCEBs using FORS2. We have found multi-component Hα emission line profiles in six of our targets, indicating that multiple Hα emission sites are rather common in short-period PCEBs. The underlying physical mechanisms, however, can be fundamentally different. In our sample we find one system where the extracted radial velocities of two identified components indicate that both originate in the late-type secondary star, where one is caused by irradiation from the hot white dwarf primary and the other by stellar activity. Another object presents two components that are located on opposite sides of the centre-of-mass, suggesting a case similar to LTT 560, i.e. that accretion of stellar wind from the secondary star produces Hα emission on, or close to, the white dwarf.

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Six detached white-dwarf close binaries

Cited by 58 publications

References 86 publications

Post common envelope binaries from the SDSS

Post common envelope binaries from the SDSS

High-resolution UVES/VLT spectra of white dwarfs observed for the ESO SN Ia Progenitor Survey

Multiple emission line components in detached post-common-envelope binaries

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